Gliese 317
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Pyxis |
| Right ascension | 08h 40m 59.2056s[1] |
| Declination | −23° 27′ 22.5986″[1] |
| Apparent magnitude (V) | 11.98
|
| Characteristics | |
| Spectral type | M2.5V[2] |
| Variable type | none reported |
| Astrometry | |
| Radial velocity (Rv) | 87.8[2] km/s |
| Proper motion (μ) | RA: −461.162±0.139[1] mas/yr Dec.: 805.571±0.126[1] mas/yr |
| Parallax (π) | 65.7744 ± 0.0557 mas[1] |
| Distance | 49.59 ± 0.04 ly (15.20 ± 0.01 pc) |
| Other designations | |
| Details | |
| Mass | 0.42 ± 0.05[2] M☉ |
| Temperature | 3510 ± 50[2] K |
| Metallicity [Fe/H] | +0.3[2][3] dex |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
Gliese 317 is a red dwarf approximately 50 light-years away in the constellation of Pyxis. As of 2011[update], two extrasolar planets have been confirmed to be orbiting the star.[2][4] Photometric calibrations and infrared spectroscopic measurements[3] indicate that the star is enriched in heavy elements compared to the Sun.
Planetary system
In 2007, a jovian planet (designated Gliese 317 b) was announced to orbit the star.[4] The planet orbits about 95% the distance between Earth to the Sun. Despite of this, it takes about 1.9 years, due to the lower mass of the central M dwarf. Astrometric measurements on Gliese 317 provided a significant update to the distance, putting the star at 15.3 pc, which is 65% further out than previously assumed.[2] Using mass-luminosity calibrations, the new distance implies the star is significantly more massive and so are the planet candidates. The same astrometric measurements allowed to constrain the orbital inclination and put an upper limit to the mass of Gliese 317 b (98% confidence level) of 2.5 MJ.
The second planet in the system was also confirmed with the additional new RV measurements, but the period and orbital parameters of Gliese 317 c are still very uncertain (P>2000 days).[2] A stability analysis on this putative system suggest that the pair of gas giant planets are in a 4:1 mean motion resonance.[5] The second planet, remote from its host star, is a good candidate for direct imaging.[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >1.81 ± 0.05 MJ | 1.148 | 692.0 ± 2 | 0.11 ± 0.05 | — | — |
| c (unconfirmed) | ≥1.6 MJ | ≥5.5 | ≥7100 | unknown | — | — |
See also
References
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d e f g h i j Anglada-Escude, Guillem; et al. (2012), "Astrometry and radial velocities of the planet host M dwarf Gliese 317: new trigonometric distance, metallicity and upper limit to the mass of Gliese 317 b", The Astrophysical Journal, 764 (1): 37A, arXiv:1111.2623, Bibcode:2012ApJ...746...37A, doi:10.1088/0004-637X/746/1/37, S2CID 118526264
- ^ a b Terrien, Ryan C.; et al. (2012), "An H-band Spectroscopic Metallicity Calibration for M Dwarfs", The Astrophysical Journal, 747 (2): L38, arXiv:1202.1800, Bibcode:2012ApJ...747L..38T, doi:10.1088/2041-8205/747/2/L38, S2CID 118403568
- ^ a b Johnson, J. A.; et al. (2007), "A New Planet Around an M Dwarf: Revealing a Correlation between Exoplanets and Stellar Mass", The Astrophysical Journal, 670 (1): 833–840, arXiv:0707.2409, Bibcode:2007ApJ...670..833J, doi:10.1086/521720, S2CID 9135084
- ^ Rory Barnes; Richard Greenberg (2008). "Extrasolar Planet Interactions". Proceedings of the International Astronomical Union. 3: 469–478. arXiv:0801.3226v1. Bibcode:2008IAUS..249..469B. doi:10.1017/S1743921308016980. S2CID 17096607.
External links
- "Notes for star GJ 317". The Extrasolar Planet Encyclopedia. Retrieved 9 August 2008.
- Extrasolar Planet Interactions by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
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